A close-up look at the whirlpool around a gigantic black hole
More than 50 years ago, the astronomer Maarten Schmidt identified the first “quasi-stellar object” or quasar, named 3C 273, as an extremely bright but distant object. The energy emitted by such a quasar is much greater than in a normal galaxy such as our Milky Way and cannot be produced by regular fusion processes in stars. Instead, astronomers assume that gravitational energy is converted into heat as material is being swallowed by an extremely massive black hole.
An international team of astronomers has now used the GRAVITY instrument to look deep into the heart of the quasar and was able to actually observe the structure of rapidly moving gas around the central black hole. So far, such observations had not been possible due to the small angular size of this inner region, which is about the size of our Solar system but at a distance of some 2.5 billion lightyears. The GRAVITY instrument combines all four ESO VLT telescopes in a technique called interferometry, which allows a huge gain in angular resolution, equivalent to a telescope with 130 metres in diameter. Thus the astronomers can reveal structures at the level of 10 micro-arcseconds, which corresponds to about 0.1 lightyears at the distance of the quasar (or an object the size of a 1-Euro-coin on the Moon).
“GRAVITY allowed us to resolve the so-called ‘broad line region’ for the first time ever, and to observe the motion of gas clouds around the central black hole”, explains Eckhard Sturm, lead author from the Max Planck Institute for Extraterrestrial Physics (MPE). “Our observations reveal that the gas clouds do whirl around the central black hole.”
The broad atomic emission lines are an observational hallmark of quasars, clearly indicating the extra-galactic origin of the source. So far, the size of the broad line region is measured mainly by a method called “reverberation mapping”. Brightness variations of the quasar’s central engine cause a light echo once the radiation hits clouds further out – the larger the size of the system, the later the echo. In the best cases, the motions of the gas can also be identified, often implying a disk in rotation. This result, derived from timing information, can now be confronted with spatially resolved observations with GRAVITY.
“Our results support the fundamental assumptions of reverberation mapping,” confirms Jason Dexter, co-lead author from MPE. “Information about the motion and size of the region immediately around the black hole are crucial to measure its mass,” he adds. For the first time, the method was now tested experimentally and passed its test with flying colours, confirming previous mass estimates of about 300 million solar masses for the black hole. Thus, GRAVITY provides both a confirmation of the main method used previously to determine black hole masses in quasars and a new and highly accurate, independent method to measure such masses. It thereby promises to provide a benchmark for measuring black hole masses in thousands of other quasars.
Quasars play a fundamental role in the history of the Universe, as their evolution is intricately tied to galaxy growth. While astronomers assume that basically all large galaxies harbour a massive black hole at their centre, so far only the one in our Milky Way has been accessible for detailed studies.
“This is the first time that we can spatially resolve and study the immediate environs of a massive black hole outside our home galaxy, the Milky Way,” emphasizes Reinhard Genzel, head of the infrared research group at MPE. “Black holes are intriguing objects, allowing us to probe physics under extreme conditions – and with GRAVITY we can now probe them both near and far.”
Zoom into the centre of the quasar 3C273
This animation shows a zoom from an optical image of the quasar to an artist’s impression of the surroundings of a supermassive black hole, composed of a dusty torus, very hot, infalling material and often a jet of material ejected at high speeds from the black hole’s poles. Astronomers were now able to spatially resolve the “broad line region”, where gas clouds whirl around the central black hole.
1. Quasars or “quasi-stellar objects” are the active nuclei of far-away galaxies, which are extremely luminous. They typically appear as bright as several hundred billion stars, ten times more luminous than all stars in our Milky Way combined. This extreme luminosity allows them to be observed to vast distances; quasars are among the most distant astronomical objects that can be observed.
2. 3C273 was the first quasar to be identified as a “quasi-stellar object” by Maarten Schmidt in 1963. It is located in the constellation Virgo and can even be observed with good amateur telescopes.
3. The method of “reverberation mapping” is used in estimating the mass of the central black hole in a quasar. Typically, the continuum radiation from the inner accretion disk, where in-falling material is heated to very high temperature, is variable. This continuum radiation can be observed directly, but it also illuminates gas clouds a bit further away from the centre. These clouds in turn will send out radiation in emission lines, which are broadened due to their fast rotation (the “broad line region”). The time delay between the variability of the continuum (from matter close to the black hole) and the broad line region a bit further out serves as a characteristic length scale – on the order of 1 lightmonth or the size of our Solar System. The length scale thus provides information on the geometry around the black hole and can be used to estimate its mass.
4. The GRAVITY instrument combines the light from the four ESO VLT telescopes on Paranal, Chile, to form a virtual telescope with 130 metres across, using a technique called interferometry. This enables the astronomers to detect much finer detail in astronomical objects than is possible with a single telescope.
5. The results are presented in a Nature paper by the GRAVITY collaboration: E. Sturm (Max Planck Institute for Extraterrestrial Physics [MPE]), J. Dexter (MPE), O. Pfuhl (MPE), M. R. Stock (MPE), R. I. Davies (MPE), D. Lutz (MPE), Y. Clénet (LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Univ. Paris Diderot, Sorbonne Paris Cité [LESIA])), A. Eckart (University of Cologne; Max Planck Institute for Radio Astronomy), F. Eisenhauer (MPE), R. Genzel (MPE; University of California), D. Gratadour (LESIA), S. F. Hönig (Department of Physics and Astronomy, University of Southampton), M. Kishimoto (Department of Physics, Kyoto Sangyo University), S. Lacour (LESIA), F. Millour (Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS), H. Netzer (School of Physics and Astronomy, Tel Aviv University), G. Perrin (LESIA), B. M. Peterson (Department of Astronomy, Ohio State University, Center for Cosmology and AstroParticle Physics, Ohio State University, Space Telescope Science Institute), P.O. Petrucci (Univ. Grenoble Alpes, CNRS, IPAG [IPAG]), D. Rouan (LESIA), I. Waisberg (MPE), J. Woillez (ESO, Garching, Germany), A. Amorim (CENTRA and Universidade de Lisboa), W. Brandner (Max Planck Institute for Astronomy), N. M. Förster Schreiber (MPE), P. J. V. Garcia (CENTRA and Universidade do Porto, ESO, Santiago, Chile), S. Gillessen (MPE), T. Ott (MPE), T. Paumard (LESIA), K. Perraut (IPAG), S. Scheithauer (Max Planck Institute for Astronomy), C. Straubmeier (1. Physikalisches Institut, Universität zu Köln), L. J. Tacconi (MPE), F. Widmann (MPE)